Infrared observations of the 2006 outburst of the recurrent nova RS Ophiuchi: the early phase

T. Kerr; B. Yang; Y. Matsuoka; Y. Tsuzuki; M. F. Bode; S. P. S. Eyres; T. R. Geballe; C. E. Woodward; R. D. Gehrz; D. K. Lynch; Richard J. Rudy; Ray W. Russell; Tim J. O'brien; S. G. Starrfield; R. J. Davis; J.-u. Ness; Jeremy J. Drake; J. P. Osborne; K. L. Page; A. Adamson; G. Schwarz; J. Krautter; A. Evans

doi:10.1111/j.1745-3933.2006.00252.x

Infrared observations of the 2006 outburst of the recurrent nova RS Ophiuchi: the early phase

T. Kerr, B. Yang, Y. Matsuoka, Y. Tsuzuki, M. F. Bode, S. P. S. Eyres, T. R. Geballe, C. E. Woodward, R. D. Gehrz, D. K. Lynch, Richard J. Rudy, Ray W. Russell, Tim J. O'brien, S. G. Starrfield, R. J. Davis, J.-u. Ness, Jeremy J. Drake, J. P. Osborne, K. L. Page, A. AdamsonG. Schwarz, J. Krautter, A. Evans

Faculty of Computing, Engineering and Science

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Abstract

We present infrared spectroscopy of the recurrent nova RS Ophiuchi, obtained 11.81, 20.75 and 55.71 days following its 2006 eruption. The spectra are dominated by hydrogen recombination lines, together with HeI, OI and OII lines; the electron temperature of ~10^4 K implied by the recombination spectrum suggests that we are seeing primarily the wind of the red giant, ionized by the ultraviolet flash when RS Oph erupted. However, strong coronal emission lines (i.e. emission from fine structure transitions in ions having high ionization potential) are present in the last spectrum. These imply a temperature of 930000K for the coronal gas; this is in line with x-ray observations of the 2006 eruption. The emission line widths decrease with time in a way that is consistent with the shock model for the x-ray emission.

Original language	English
Pages (from-to)	L1-L5
Journal	Monthly Notices of the Royal Astronomical Society: Letters
Volume	374
Issue number	1
DOIs	https://doi.org/10.1111/j.1745-3933.2006.00252.x
Publication status	Published - 1 Jan 2007

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Kerr, T., Yang, B., Matsuoka, Y., Tsuzuki, Y., Bode, M. F., Eyres, S. P. S., Geballe, T. R., Woodward, C. E., Gehrz, R. D., Lynch, D. K., Rudy, R. J., Russell, R. W., O'brien, T. J., Starrfield, S. G., Davis, R. J., Ness, J., Drake, J. J., Osborne, J. P., Page, K. L., ... Evans, A. (2007). Infrared observations of the 2006 outburst of the recurrent nova RS Ophiuchi: the early phase. Monthly Notices of the Royal Astronomical Society: Letters, 374(1), L1-L5. https://doi.org/10.1111/j.1745-3933.2006.00252.x

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title = "Infrared observations of the 2006 outburst of the recurrent nova RS Ophiuchi: the early phase",

abstract = "We present infrared spectroscopy of the recurrent nova RS Ophiuchi, obtained 11.81, 20.75 and 55.71 days following its 2006 eruption. The spectra are dominated by hydrogen recombination lines, together with HeI, OI and OII lines; the electron temperature of ~10^4 K implied by the recombination spectrum suggests that we are seeing primarily the wind of the red giant, ionized by the ultraviolet flash when RS Oph erupted. However, strong coronal emission lines (i.e. emission from fine structure transitions in ions having high ionization potential) are present in the last spectrum. These imply a temperature of 930000K for the coronal gas; this is in line with x-ray observations of the 2006 eruption. The emission line widths decrease with time in a way that is consistent with the shock model for the x-ray emission.",

author = "T. Kerr and B. Yang and Y. Matsuoka and Y. Tsuzuki and Bode, {M. F.} and Eyres, {S. P. S.} and Geballe, {T. R.} and Woodward, {C. E.} and Gehrz, {R. D.} and Lynch, {D. K.} and Rudy, {Richard J.} and Russell, {Ray W.} and O'brien, {Tim J.} and Starrfield, {S. G.} and Davis, {R. J.} and J.-u. Ness and Drake, {Jeremy J.} and Osborne, {J. P.} and Page, {K. L.} and A. Adamson and G. Schwarz and J. Krautter and A. Evans",

year = "2007",

month = jan,

day = "1",

doi = "10.1111/j.1745-3933.2006.00252.x",

language = "English",

volume = "374",

pages = "L1--L5",

journal = "Monthly Notices of the Royal Astronomical Society: Letters",

issn = "1745-3925",

publisher = "Oxford University Press",

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Kerr, T, Yang, B, Matsuoka, Y, Tsuzuki, Y, Bode, MF, Eyres, SPS, Geballe, TR, Woodward, CE, Gehrz, RD, Lynch, DK, Rudy, RJ, Russell, RW, O'brien, TJ, Starrfield, SG, Davis, RJ, Ness, J, Drake, JJ, Osborne, JP, Page, KL, Adamson, A, Schwarz, G, Krautter, J & Evans, A 2007, 'Infrared observations of the 2006 outburst of the recurrent nova RS Ophiuchi: the early phase', Monthly Notices of the Royal Astronomical Society: Letters, vol. 374, no. 1, pp. L1-L5. https://doi.org/10.1111/j.1745-3933.2006.00252.x

TY - JOUR

T1 - Infrared observations of the 2006 outburst of the recurrent nova RS Ophiuchi: the early phase

AU - Kerr, T.

AU - Yang, B.

AU - Matsuoka, Y.

AU - Tsuzuki, Y.

AU - Bode, M. F.

AU - Eyres, S. P. S.

AU - Geballe, T. R.

AU - Woodward, C. E.

AU - Gehrz, R. D.

AU - Lynch, D. K.

AU - Rudy, Richard J.

AU - Russell, Ray W.

AU - O'brien, Tim J.

AU - Starrfield, S. G.

AU - Davis, R. J.

AU - Ness, J.-u.

AU - Drake, Jeremy J.

AU - Osborne, J. P.

AU - Page, K. L.

AU - Adamson, A.

AU - Schwarz, G.

AU - Krautter, J.

AU - Evans, A.

PY - 2007/1/1

Y1 - 2007/1/1

N2 - We present infrared spectroscopy of the recurrent nova RS Ophiuchi, obtained 11.81, 20.75 and 55.71 days following its 2006 eruption. The spectra are dominated by hydrogen recombination lines, together with HeI, OI and OII lines; the electron temperature of ~10^4 K implied by the recombination spectrum suggests that we are seeing primarily the wind of the red giant, ionized by the ultraviolet flash when RS Oph erupted. However, strong coronal emission lines (i.e. emission from fine structure transitions in ions having high ionization potential) are present in the last spectrum. These imply a temperature of 930000K for the coronal gas; this is in line with x-ray observations of the 2006 eruption. The emission line widths decrease with time in a way that is consistent with the shock model for the x-ray emission.

AB - We present infrared spectroscopy of the recurrent nova RS Ophiuchi, obtained 11.81, 20.75 and 55.71 days following its 2006 eruption. The spectra are dominated by hydrogen recombination lines, together with HeI, OI and OII lines; the electron temperature of ~10^4 K implied by the recombination spectrum suggests that we are seeing primarily the wind of the red giant, ionized by the ultraviolet flash when RS Oph erupted. However, strong coronal emission lines (i.e. emission from fine structure transitions in ions having high ionization potential) are present in the last spectrum. These imply a temperature of 930000K for the coronal gas; this is in line with x-ray observations of the 2006 eruption. The emission line widths decrease with time in a way that is consistent with the shock model for the x-ray emission.

U2 - 10.1111/j.1745-3933.2006.00252.x

DO - 10.1111/j.1745-3933.2006.00252.x

M3 - Article

SN - 1745-3925

VL - 374

SP - L1-L5

JO - Monthly Notices of the Royal Astronomical Society: Letters

JF - Monthly Notices of the Royal Astronomical Society: Letters

IS - 1

ER -

Infrared observations of the 2006 outburst of the recurrent nova RS Ophiuchi: the early phase

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